The Atacama Cosmology Telescope: CMB polarization at 200 < l < 9000

被引：149

作者：

Naess, Sigurd ^{[1
]}

Hasselfield, Matthew ^{[2
,3
]}

McMahon, Jeff ^{[4
]}

Niemack, Michael D. ^{[5
]}

Addison, Graeme E. ^{[3
]}

Ade, Peter A. R. ^{[6
]}

Allison, Rupert ^{[1
]}

Amiri, Mandana ^{[3
]}

Battaglia, Nick ^{[7
]}

Beall, James A. ^{[8
]}

de Bernardis, Francesco ^{[5
]}

Bond, J. Richard ^{[9
]}

Britton, Joe ^{[8
]}

Calabrese, Erminia ^{[1
]}

Cho, Hsiao-mei ^{[8
]}

Coughlin, Kevin ^{[4
]}

Crichton, Devin ^{[10
]}

Das, Sudeep ^{[11
]}

Datta, Rahul ^{[4
]}

Devlin, Mark J. ^{[12
]}

Dicker, Simon R. ^{[12
]}

Dunkley, Joanna ^{[1
]}

Duenner, Rolando ^{[13
]}

Fowler, Joseph W. ^{[8
]}

Fox, Anna E. ^{[8
]}

Gallardo, Patricio ^{[5
,13
]}

Grace, Emily ^{[14
]}

Gralla, Megan ^{[10
]}

Hajian, Amir ^{[9
]}

Halpern, Mark ^{[3
]}

Henderson, Shawn ^{[5
]}

Hill, J. Colin ^{[2
]}

Hilton, Gene C. ^{[8
]}

Hilton, Matt ^{[15
]}

Hincks, Adam D. ^{[3
]}

Hlozek, Renee ^{[2
]}

Ho, Patty ^{[14
]}

Hubmayr, Johannes ^{[8
]}

Huffenberger, Kevin M. ^{[16
]}

Hughes, John P. ^{[17
]}

Infante, Leopoldo ^{[13
]}

Irwin, Kent ^{[18
]}

Jackson, Rebecca ^{[4
,19
]}

Kasanda, Simon Muya ^{[15
,20
]}

Klein, Jeff ^{[12
]}

Koopman, Brian ^{[5
]}

Kosowsky, Arthur ^{[21
]}

Li, Dale ^{[8
]}

Louis, Thibaut

Lungu, Marius ^{[12
]}

机构：

[1] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England

[2] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[3] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada

[4] Univ Michigan, Dept Phys, Ann Arbor, MI 48103 USA

[5] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA

[6] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[7] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA

[8] NIST Quantum Devices Grp, Boulder, CO 80305 USA

[9] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada

[10] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[11] Argonne Natl Lab, Dept High Energy Phys, Argonne, IL 60439 USA

[12] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[13] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago 22, Chile

[14] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA

[15] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa

[16] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA

[17] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA

[18] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[19] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA

[20] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa

[21] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA

[22] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA

[23] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA

[24] Univ Illinois, Dept Astron, Urbana, IL 61801 USA

[25] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA

[26] Sociedad Radiosky Asesoras Ingn Ltd Lincoyan, Concepcion, Chile

[27] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA

[28] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[29] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[30] Univ Penn, Dept Phys, W Chester, PA 19383 USA

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2014年 / 10期

基金：

美国国家科学基金会; 加拿大创新基金会;

关键词：

CMBR polarisation; CMBR experiments; cosmological parameters from CMBR; CMBR detectors; PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND POLARIZATION; POWER SPECTRUM; CRAB-NEBULA; CONSTRAINTS; PARAMETERS; CATALOG; MAPS;

D O I：

10.1088/1475-7516/2014/10/007

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on measurements of the cosmic microwave background (CMB) and celestial polarization at 146 GHz made with the Atacama Cosmology Telescope Polarimeter (ACTPol) in its first three months of observing. Four regions of sky covering a total of 270 square degrees were mapped with an angular resolution of 1.3'. The map noise levels in the four regions are between 11 and 17 mu K-arcmin. We present TT, TE, EE, TB, EB, and BB power spectra from three of these regions. The observed E-mode polarization power spectrum, displaying six acoustic peaks in the range 200 < l < 3000, is an excellent fit to the prediction of the best-fit cosmological models from WMAP9+ACT and Planck data. The polarization power spectrum, which mainly reflects primordial plasma velocity perturbations, provides an independent determination of cosmological parameters consistent with those based on the temperature power spectrum, which results mostly from primordial density perturbations. We find that without masking any point sources in the EE data at l < 9000, the Poisson tail of the EE power spectrum due to polarized point sources has an amplitude less than 2.4 mu K-2 at l = 3000 at 95% confidence. Finally, we report that the Crab Nebula, an important polarization calibration source at microwave frequencies, has 8.7% polarization with an angle of 150.7 degrees +/- 0.6 degrees when smoothed with a 5' Gaussian beam.

引用

页数：32

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The Atacama Cosmology Telescope: CMB polarization at 200 &lt; l &lt; 9000

The Atacama Cosmology Telescope: CMB polarization at 200 < l < 9000